Parameters of the WR features in the optical spectrum of the CSPN of NGC 6905.
ID . | Nature . | Ion . | λ0 . | χ . | λc . | F† . | FWHM . | EW . | SNR . | Fλ/FRB . | EWλ/EWRB . |
---|---|---|---|---|---|---|---|---|---|---|---|
. | . | . | (Å) . | (eV) . | (Å) . | (10−14 erg cm−2 s−1) . | (Å) . | (Å) . | . | (FRB = 100) . | (FRB = 100) . |
(1) . | (2) . | (3) . | (4) . | (5) . | (6) . | (7) . | (8) . | (9) . | (10) . | (11) . | (12) . |
VB | |||||||||||
1 | WR | O vi | 3811 | 138.1 | 3811.0 | 206.99 ± 0.46 | 24.8 | 245.9 ± 1.3 | 43.6 | 572.74 ± 2.29 | 279.37 ± 0.15 |
2 | WR | O vi | 3834 | 138.1 | 3834.0 | 90.25 ± 0.36 | 23.9 | 102.7 ± 0.6 | 43.6 | 249.72 ± 1.30 | 116.69 ± 0.19 |
BB | |||||||||||
3 | WR | C iv | 4658 | 64.5 | 4658.0 | 53.95 ± 0.59 | 27.8 | 77.1 ± 1.1 | 20.2 | 149.28 ± 1.71 | 87.55 ± 0.86 |
4 | WR | He ii | 4686 | 24.6 | 4686.0 | 61.52 ± 0.58 | 25.4 | 90.4 ± 1.2 | 20.2 | 170.23 ± 1.70 | 102.71 ± 0.94 |
5 | Neb | He ii | 4686 | 24.6 | 4686.1 | 8.62 ± 0.24 | 5.4 | 12.7 ± 0.4 | 20.2 | 23.85 ± 0.67 | 14.39 ± 0.45 |
6 | Neb | [Ar iv] | 4711 | 4711.0 | 1.05 ± 0.19 | 5.4 | 1.6 ± 0.3 | 20.2 | 2.91 ± 0.53 | 1.80 ± 0.32 | |
RB | |||||||||||
7 | WR | C iv | 5806 | 64.5 | 5802.8 | 36.14 ± 0.12 | 37.4 | 88.0 ± 0.4 | 65.5 | 100.00 ± 0.47 | 100.00 ± 0.03 |
other lines | |||||||||||
8 | WR | C iv | 3689 | 64.5 | 3689.0 | 5.06 ± 0.20 | 14.4 | 5.7 ± 0.2 | 43.6 | 14.00 ± 0.56 | 6.50 ± 0.22 |
9 | WR | C iv | 3933 | 64.5 | 3932.4 | 3.19 ± 0.19 | 18.1 | 4.2 ± 0.2 | 43.6 | 8.83 ± 0.53 | 4.73 ± 0.25 |
10 | WR | He ii | 4200 | 24.6 | 4200.6 | 1.29 ± 0.17 | 17.4 | 1.8 ± 0.2 | 43.6 | 3.57 ± 0.47 | 2.04 ± 0.25 |
11 | WR | C iv | 4227 | 64.5 | 4226.7 | 2.96 ± 0.18 | 18.9 | 4.2 ± 0.2 | 43.6 | 8.19 ± 0.50 | 4.72 ± 0.26 |
12 | WR | C iv | 4440 | 64.5 | 4442.8 | 1.95 ± 0.28 | 11.0 | 2.9 ± 0.4 | 20.2 | 5.40 ± 0.77 | 3.30 ± 0.45 |
13 | WR | O vi | 4500 | 138.1 | 4498.1 | 5.48 ± 0.27 | 8.9 | 8.2 ± 0.4 | 20.2 | 15.16 ± 0.75 | 9.34 ± 0.43 |
14 | WR | He ii | 4541 | 24.6 | 4541.0 | 5.19 ± 0.45 | 29.9 | 7.8 ± 0.7 | 20.2 | 14.36 ± 1.25 | 8.89 ± 0.73 |
15 | WR | C iv | 4789 | 64.5 | 4789.2 | 1.99 ± 0.33 | 21.4 | 3.4 ± 0.6 | 20.2 | 5.51 ± 0.91 | 3.84 ± 0.62 |
16 | WR | O v | 4933 | 113.9 | 4933.1 | 4.87 ± 0.38 | 30.3 | 8.7 ± 0.7 | 20.2 | 13.48 ± 1.05 | 9.92 ± 0.74 |
17 | WR | O v | 5100 | 113.9 | 5100.0 | 3.60 ± 0.41 | 41.5 | 6.9 ± 0.8 | 20.2 | 9.96 ± 1.14 | 7.84 ± 0.86 |
18 | WR | O vi | 5166 | 138.1 | 5166.5 | 0.52 ± 0.06 | 11.4 | 1.0 ± 0.1 | 20.2 | 1.44 ± 0.17 | 1.15 ± 0.13 |
19 | WR | O vi | 5290 | 138.1 | 5288.9 | 13.13 ± 0.09 | 17.3 | 26.4 ± 0.2 | 66.8 | 36.33 ± 0.28 | 29.94 ± 0.09 |
20 | WR | He ii | 5412 | 24.6 | 5411.8 | 8.49 ± 0.09 | 23.6 | 17.9 ± 0.2 | 66.8 | 23.49 ± 0.26 | 20.34 ± 0.13 |
21 | WR | C iv | 5470 | 64.5 | 5468.6 | 6.89 ± 0.10 | 26.6 | 114.9 ± 0.2 | 66.8 | 19.07 ± 0.26 | 16.91 ± 0.15 |
22 | WR | O v | 5600 | 113.9 | 5595.0 | 2.59 ± 0.07 | 35.5 | 5.9 ± 0.2 | 65.5 | 7.17 ± 0.28 | 6.72 ± 0.22 |
23 | WR | O vi | 6200 | 138.1 | 6198.5 | 3.35 ± 0.08 | 19.0 | 10.2 ± 0.3 | 43.3 | 9.27 ± 0.22 | 11.61 ± 0.24 |
24 | WR | He ii | 6406 | 24.6 | 6406.0 | 0.63 ± 0.03 | 11.8 | 2.2 ± 0.2 | 43.3 | 1.74 ± 0.14 | 2.51 ± 0.20 |
25 | WR | He ii | 6560 | 24.6 | 6557.7 | 10.95 ± 0.07 | 44.5 | 36.7 ± 0.4 | 43.3 | 30.30 ± 0.35 | 41.69 ± 0.29 |
26 | WR | O v | 6740 | 113.9 | 6746.3 | 1.33 ± 0.10 | 47.9 | 5.3 ± 0.4 | 43.3 | 3.68 ± 0.26 | 6.01 ± 0.40 |
27 | WR | C iv | 7060 | 64.5 | 7059.9 | 8.54 ± 0.04 | 35.4 | 39.0 ± 0.3 | 57.9 | 23.63 ± 0.18 | 44.31 ± 0.15 |
Special lines|$^{\dagger }\, ^{\dagger }$| | |||||||||||
28 | stellar emission | Ne vii | 4555 | 207.3 | 4552.5 | 1.14 ± 0.30 | 14.4 | 1.7 ± 0.5 | 20.2 | 3.15 ± 0.83 | 1.96 ± 0.51 |
29 | stellar emission | Ne vii | 5666 | 207.3 | 5665.4 | 1.63 ± 0.07 | 20.4 | 3.8 ± 0.2 | 65.5 | 4.51 ± 0.19 | 4.36 ± 0.17 |
30 | stellar emission | Ne viii | 6068 | 239.1 | 6065.9 | 1.51 ± 0.07 | 12.1 | 4.2 ± 0.2 | 43.3 | 4.18 ± 0.19 | 4.82 ± 0.21 |
ID . | Nature . | Ion . | λ0 . | χ . | λc . | F† . | FWHM . | EW . | SNR . | Fλ/FRB . | EWλ/EWRB . |
---|---|---|---|---|---|---|---|---|---|---|---|
. | . | . | (Å) . | (eV) . | (Å) . | (10−14 erg cm−2 s−1) . | (Å) . | (Å) . | . | (FRB = 100) . | (FRB = 100) . |
(1) . | (2) . | (3) . | (4) . | (5) . | (6) . | (7) . | (8) . | (9) . | (10) . | (11) . | (12) . |
VB | |||||||||||
1 | WR | O vi | 3811 | 138.1 | 3811.0 | 206.99 ± 0.46 | 24.8 | 245.9 ± 1.3 | 43.6 | 572.74 ± 2.29 | 279.37 ± 0.15 |
2 | WR | O vi | 3834 | 138.1 | 3834.0 | 90.25 ± 0.36 | 23.9 | 102.7 ± 0.6 | 43.6 | 249.72 ± 1.30 | 116.69 ± 0.19 |
BB | |||||||||||
3 | WR | C iv | 4658 | 64.5 | 4658.0 | 53.95 ± 0.59 | 27.8 | 77.1 ± 1.1 | 20.2 | 149.28 ± 1.71 | 87.55 ± 0.86 |
4 | WR | He ii | 4686 | 24.6 | 4686.0 | 61.52 ± 0.58 | 25.4 | 90.4 ± 1.2 | 20.2 | 170.23 ± 1.70 | 102.71 ± 0.94 |
5 | Neb | He ii | 4686 | 24.6 | 4686.1 | 8.62 ± 0.24 | 5.4 | 12.7 ± 0.4 | 20.2 | 23.85 ± 0.67 | 14.39 ± 0.45 |
6 | Neb | [Ar iv] | 4711 | 4711.0 | 1.05 ± 0.19 | 5.4 | 1.6 ± 0.3 | 20.2 | 2.91 ± 0.53 | 1.80 ± 0.32 | |
RB | |||||||||||
7 | WR | C iv | 5806 | 64.5 | 5802.8 | 36.14 ± 0.12 | 37.4 | 88.0 ± 0.4 | 65.5 | 100.00 ± 0.47 | 100.00 ± 0.03 |
other lines | |||||||||||
8 | WR | C iv | 3689 | 64.5 | 3689.0 | 5.06 ± 0.20 | 14.4 | 5.7 ± 0.2 | 43.6 | 14.00 ± 0.56 | 6.50 ± 0.22 |
9 | WR | C iv | 3933 | 64.5 | 3932.4 | 3.19 ± 0.19 | 18.1 | 4.2 ± 0.2 | 43.6 | 8.83 ± 0.53 | 4.73 ± 0.25 |
10 | WR | He ii | 4200 | 24.6 | 4200.6 | 1.29 ± 0.17 | 17.4 | 1.8 ± 0.2 | 43.6 | 3.57 ± 0.47 | 2.04 ± 0.25 |
11 | WR | C iv | 4227 | 64.5 | 4226.7 | 2.96 ± 0.18 | 18.9 | 4.2 ± 0.2 | 43.6 | 8.19 ± 0.50 | 4.72 ± 0.26 |
12 | WR | C iv | 4440 | 64.5 | 4442.8 | 1.95 ± 0.28 | 11.0 | 2.9 ± 0.4 | 20.2 | 5.40 ± 0.77 | 3.30 ± 0.45 |
13 | WR | O vi | 4500 | 138.1 | 4498.1 | 5.48 ± 0.27 | 8.9 | 8.2 ± 0.4 | 20.2 | 15.16 ± 0.75 | 9.34 ± 0.43 |
14 | WR | He ii | 4541 | 24.6 | 4541.0 | 5.19 ± 0.45 | 29.9 | 7.8 ± 0.7 | 20.2 | 14.36 ± 1.25 | 8.89 ± 0.73 |
15 | WR | C iv | 4789 | 64.5 | 4789.2 | 1.99 ± 0.33 | 21.4 | 3.4 ± 0.6 | 20.2 | 5.51 ± 0.91 | 3.84 ± 0.62 |
16 | WR | O v | 4933 | 113.9 | 4933.1 | 4.87 ± 0.38 | 30.3 | 8.7 ± 0.7 | 20.2 | 13.48 ± 1.05 | 9.92 ± 0.74 |
17 | WR | O v | 5100 | 113.9 | 5100.0 | 3.60 ± 0.41 | 41.5 | 6.9 ± 0.8 | 20.2 | 9.96 ± 1.14 | 7.84 ± 0.86 |
18 | WR | O vi | 5166 | 138.1 | 5166.5 | 0.52 ± 0.06 | 11.4 | 1.0 ± 0.1 | 20.2 | 1.44 ± 0.17 | 1.15 ± 0.13 |
19 | WR | O vi | 5290 | 138.1 | 5288.9 | 13.13 ± 0.09 | 17.3 | 26.4 ± 0.2 | 66.8 | 36.33 ± 0.28 | 29.94 ± 0.09 |
20 | WR | He ii | 5412 | 24.6 | 5411.8 | 8.49 ± 0.09 | 23.6 | 17.9 ± 0.2 | 66.8 | 23.49 ± 0.26 | 20.34 ± 0.13 |
21 | WR | C iv | 5470 | 64.5 | 5468.6 | 6.89 ± 0.10 | 26.6 | 114.9 ± 0.2 | 66.8 | 19.07 ± 0.26 | 16.91 ± 0.15 |
22 | WR | O v | 5600 | 113.9 | 5595.0 | 2.59 ± 0.07 | 35.5 | 5.9 ± 0.2 | 65.5 | 7.17 ± 0.28 | 6.72 ± 0.22 |
23 | WR | O vi | 6200 | 138.1 | 6198.5 | 3.35 ± 0.08 | 19.0 | 10.2 ± 0.3 | 43.3 | 9.27 ± 0.22 | 11.61 ± 0.24 |
24 | WR | He ii | 6406 | 24.6 | 6406.0 | 0.63 ± 0.03 | 11.8 | 2.2 ± 0.2 | 43.3 | 1.74 ± 0.14 | 2.51 ± 0.20 |
25 | WR | He ii | 6560 | 24.6 | 6557.7 | 10.95 ± 0.07 | 44.5 | 36.7 ± 0.4 | 43.3 | 30.30 ± 0.35 | 41.69 ± 0.29 |
26 | WR | O v | 6740 | 113.9 | 6746.3 | 1.33 ± 0.10 | 47.9 | 5.3 ± 0.4 | 43.3 | 3.68 ± 0.26 | 6.01 ± 0.40 |
27 | WR | C iv | 7060 | 64.5 | 7059.9 | 8.54 ± 0.04 | 35.4 | 39.0 ± 0.3 | 57.9 | 23.63 ± 0.18 | 44.31 ± 0.15 |
Special lines|$^{\dagger }\, ^{\dagger }$| | |||||||||||
28 | stellar emission | Ne vii | 4555 | 207.3 | 4552.5 | 1.14 ± 0.30 | 14.4 | 1.7 ± 0.5 | 20.2 | 3.15 ± 0.83 | 1.96 ± 0.51 |
29 | stellar emission | Ne vii | 5666 | 207.3 | 5665.4 | 1.63 ± 0.07 | 20.4 | 3.8 ± 0.2 | 65.5 | 4.51 ± 0.19 | 4.36 ± 0.17 |
30 | stellar emission | Ne viii | 6068 | 239.1 | 6065.9 | 1.51 ± 0.07 | 12.1 | 4.2 ± 0.2 | 43.3 | 4.18 ± 0.19 | 4.82 ± 0.21 |
(1) Identification number; (2) nature of the contributing emission line: WR (broad/stellar) or nebular (narrow); (3) ion; (4) rest wavelength in Å; (5) Ionization potential [eV]; (6) observed centre of the line; (7) flux [10−14 erg cm−2 s−1]; (8) full width at half-maximum (FWHM) [Å]; (9) equivalent width (EW) [Å]; (10) continuum signal-to-noise ratio (SNR) closest to the feature; (11) line fluxes normalized to that of the RB. The ratio has been computed adopting F(RB) = 100. (12) EW normalized to that of the RB, adopting EW(RB) = 100. Special lines |$^{\dagger }\, ^{\dagger }$| correspond to high ionization Ne lines from stellar emission origin (Werner, Rauch & Kruk 2007). † Only the statistical errors, determined with equations (1) and (2), are shown in this table.
Parameters of the WR features in the optical spectrum of the CSPN of NGC 6905.
ID . | Nature . | Ion . | λ0 . | χ . | λc . | F† . | FWHM . | EW . | SNR . | Fλ/FRB . | EWλ/EWRB . |
---|---|---|---|---|---|---|---|---|---|---|---|
. | . | . | (Å) . | (eV) . | (Å) . | (10−14 erg cm−2 s−1) . | (Å) . | (Å) . | . | (FRB = 100) . | (FRB = 100) . |
(1) . | (2) . | (3) . | (4) . | (5) . | (6) . | (7) . | (8) . | (9) . | (10) . | (11) . | (12) . |
VB | |||||||||||
1 | WR | O vi | 3811 | 138.1 | 3811.0 | 206.99 ± 0.46 | 24.8 | 245.9 ± 1.3 | 43.6 | 572.74 ± 2.29 | 279.37 ± 0.15 |
2 | WR | O vi | 3834 | 138.1 | 3834.0 | 90.25 ± 0.36 | 23.9 | 102.7 ± 0.6 | 43.6 | 249.72 ± 1.30 | 116.69 ± 0.19 |
BB | |||||||||||
3 | WR | C iv | 4658 | 64.5 | 4658.0 | 53.95 ± 0.59 | 27.8 | 77.1 ± 1.1 | 20.2 | 149.28 ± 1.71 | 87.55 ± 0.86 |
4 | WR | He ii | 4686 | 24.6 | 4686.0 | 61.52 ± 0.58 | 25.4 | 90.4 ± 1.2 | 20.2 | 170.23 ± 1.70 | 102.71 ± 0.94 |
5 | Neb | He ii | 4686 | 24.6 | 4686.1 | 8.62 ± 0.24 | 5.4 | 12.7 ± 0.4 | 20.2 | 23.85 ± 0.67 | 14.39 ± 0.45 |
6 | Neb | [Ar iv] | 4711 | 4711.0 | 1.05 ± 0.19 | 5.4 | 1.6 ± 0.3 | 20.2 | 2.91 ± 0.53 | 1.80 ± 0.32 | |
RB | |||||||||||
7 | WR | C iv | 5806 | 64.5 | 5802.8 | 36.14 ± 0.12 | 37.4 | 88.0 ± 0.4 | 65.5 | 100.00 ± 0.47 | 100.00 ± 0.03 |
other lines | |||||||||||
8 | WR | C iv | 3689 | 64.5 | 3689.0 | 5.06 ± 0.20 | 14.4 | 5.7 ± 0.2 | 43.6 | 14.00 ± 0.56 | 6.50 ± 0.22 |
9 | WR | C iv | 3933 | 64.5 | 3932.4 | 3.19 ± 0.19 | 18.1 | 4.2 ± 0.2 | 43.6 | 8.83 ± 0.53 | 4.73 ± 0.25 |
10 | WR | He ii | 4200 | 24.6 | 4200.6 | 1.29 ± 0.17 | 17.4 | 1.8 ± 0.2 | 43.6 | 3.57 ± 0.47 | 2.04 ± 0.25 |
11 | WR | C iv | 4227 | 64.5 | 4226.7 | 2.96 ± 0.18 | 18.9 | 4.2 ± 0.2 | 43.6 | 8.19 ± 0.50 | 4.72 ± 0.26 |
12 | WR | C iv | 4440 | 64.5 | 4442.8 | 1.95 ± 0.28 | 11.0 | 2.9 ± 0.4 | 20.2 | 5.40 ± 0.77 | 3.30 ± 0.45 |
13 | WR | O vi | 4500 | 138.1 | 4498.1 | 5.48 ± 0.27 | 8.9 | 8.2 ± 0.4 | 20.2 | 15.16 ± 0.75 | 9.34 ± 0.43 |
14 | WR | He ii | 4541 | 24.6 | 4541.0 | 5.19 ± 0.45 | 29.9 | 7.8 ± 0.7 | 20.2 | 14.36 ± 1.25 | 8.89 ± 0.73 |
15 | WR | C iv | 4789 | 64.5 | 4789.2 | 1.99 ± 0.33 | 21.4 | 3.4 ± 0.6 | 20.2 | 5.51 ± 0.91 | 3.84 ± 0.62 |
16 | WR | O v | 4933 | 113.9 | 4933.1 | 4.87 ± 0.38 | 30.3 | 8.7 ± 0.7 | 20.2 | 13.48 ± 1.05 | 9.92 ± 0.74 |
17 | WR | O v | 5100 | 113.9 | 5100.0 | 3.60 ± 0.41 | 41.5 | 6.9 ± 0.8 | 20.2 | 9.96 ± 1.14 | 7.84 ± 0.86 |
18 | WR | O vi | 5166 | 138.1 | 5166.5 | 0.52 ± 0.06 | 11.4 | 1.0 ± 0.1 | 20.2 | 1.44 ± 0.17 | 1.15 ± 0.13 |
19 | WR | O vi | 5290 | 138.1 | 5288.9 | 13.13 ± 0.09 | 17.3 | 26.4 ± 0.2 | 66.8 | 36.33 ± 0.28 | 29.94 ± 0.09 |
20 | WR | He ii | 5412 | 24.6 | 5411.8 | 8.49 ± 0.09 | 23.6 | 17.9 ± 0.2 | 66.8 | 23.49 ± 0.26 | 20.34 ± 0.13 |
21 | WR | C iv | 5470 | 64.5 | 5468.6 | 6.89 ± 0.10 | 26.6 | 114.9 ± 0.2 | 66.8 | 19.07 ± 0.26 | 16.91 ± 0.15 |
22 | WR | O v | 5600 | 113.9 | 5595.0 | 2.59 ± 0.07 | 35.5 | 5.9 ± 0.2 | 65.5 | 7.17 ± 0.28 | 6.72 ± 0.22 |
23 | WR | O vi | 6200 | 138.1 | 6198.5 | 3.35 ± 0.08 | 19.0 | 10.2 ± 0.3 | 43.3 | 9.27 ± 0.22 | 11.61 ± 0.24 |
24 | WR | He ii | 6406 | 24.6 | 6406.0 | 0.63 ± 0.03 | 11.8 | 2.2 ± 0.2 | 43.3 | 1.74 ± 0.14 | 2.51 ± 0.20 |
25 | WR | He ii | 6560 | 24.6 | 6557.7 | 10.95 ± 0.07 | 44.5 | 36.7 ± 0.4 | 43.3 | 30.30 ± 0.35 | 41.69 ± 0.29 |
26 | WR | O v | 6740 | 113.9 | 6746.3 | 1.33 ± 0.10 | 47.9 | 5.3 ± 0.4 | 43.3 | 3.68 ± 0.26 | 6.01 ± 0.40 |
27 | WR | C iv | 7060 | 64.5 | 7059.9 | 8.54 ± 0.04 | 35.4 | 39.0 ± 0.3 | 57.9 | 23.63 ± 0.18 | 44.31 ± 0.15 |
Special lines|$^{\dagger }\, ^{\dagger }$| | |||||||||||
28 | stellar emission | Ne vii | 4555 | 207.3 | 4552.5 | 1.14 ± 0.30 | 14.4 | 1.7 ± 0.5 | 20.2 | 3.15 ± 0.83 | 1.96 ± 0.51 |
29 | stellar emission | Ne vii | 5666 | 207.3 | 5665.4 | 1.63 ± 0.07 | 20.4 | 3.8 ± 0.2 | 65.5 | 4.51 ± 0.19 | 4.36 ± 0.17 |
30 | stellar emission | Ne viii | 6068 | 239.1 | 6065.9 | 1.51 ± 0.07 | 12.1 | 4.2 ± 0.2 | 43.3 | 4.18 ± 0.19 | 4.82 ± 0.21 |
ID . | Nature . | Ion . | λ0 . | χ . | λc . | F† . | FWHM . | EW . | SNR . | Fλ/FRB . | EWλ/EWRB . |
---|---|---|---|---|---|---|---|---|---|---|---|
. | . | . | (Å) . | (eV) . | (Å) . | (10−14 erg cm−2 s−1) . | (Å) . | (Å) . | . | (FRB = 100) . | (FRB = 100) . |
(1) . | (2) . | (3) . | (4) . | (5) . | (6) . | (7) . | (8) . | (9) . | (10) . | (11) . | (12) . |
VB | |||||||||||
1 | WR | O vi | 3811 | 138.1 | 3811.0 | 206.99 ± 0.46 | 24.8 | 245.9 ± 1.3 | 43.6 | 572.74 ± 2.29 | 279.37 ± 0.15 |
2 | WR | O vi | 3834 | 138.1 | 3834.0 | 90.25 ± 0.36 | 23.9 | 102.7 ± 0.6 | 43.6 | 249.72 ± 1.30 | 116.69 ± 0.19 |
BB | |||||||||||
3 | WR | C iv | 4658 | 64.5 | 4658.0 | 53.95 ± 0.59 | 27.8 | 77.1 ± 1.1 | 20.2 | 149.28 ± 1.71 | 87.55 ± 0.86 |
4 | WR | He ii | 4686 | 24.6 | 4686.0 | 61.52 ± 0.58 | 25.4 | 90.4 ± 1.2 | 20.2 | 170.23 ± 1.70 | 102.71 ± 0.94 |
5 | Neb | He ii | 4686 | 24.6 | 4686.1 | 8.62 ± 0.24 | 5.4 | 12.7 ± 0.4 | 20.2 | 23.85 ± 0.67 | 14.39 ± 0.45 |
6 | Neb | [Ar iv] | 4711 | 4711.0 | 1.05 ± 0.19 | 5.4 | 1.6 ± 0.3 | 20.2 | 2.91 ± 0.53 | 1.80 ± 0.32 | |
RB | |||||||||||
7 | WR | C iv | 5806 | 64.5 | 5802.8 | 36.14 ± 0.12 | 37.4 | 88.0 ± 0.4 | 65.5 | 100.00 ± 0.47 | 100.00 ± 0.03 |
other lines | |||||||||||
8 | WR | C iv | 3689 | 64.5 | 3689.0 | 5.06 ± 0.20 | 14.4 | 5.7 ± 0.2 | 43.6 | 14.00 ± 0.56 | 6.50 ± 0.22 |
9 | WR | C iv | 3933 | 64.5 | 3932.4 | 3.19 ± 0.19 | 18.1 | 4.2 ± 0.2 | 43.6 | 8.83 ± 0.53 | 4.73 ± 0.25 |
10 | WR | He ii | 4200 | 24.6 | 4200.6 | 1.29 ± 0.17 | 17.4 | 1.8 ± 0.2 | 43.6 | 3.57 ± 0.47 | 2.04 ± 0.25 |
11 | WR | C iv | 4227 | 64.5 | 4226.7 | 2.96 ± 0.18 | 18.9 | 4.2 ± 0.2 | 43.6 | 8.19 ± 0.50 | 4.72 ± 0.26 |
12 | WR | C iv | 4440 | 64.5 | 4442.8 | 1.95 ± 0.28 | 11.0 | 2.9 ± 0.4 | 20.2 | 5.40 ± 0.77 | 3.30 ± 0.45 |
13 | WR | O vi | 4500 | 138.1 | 4498.1 | 5.48 ± 0.27 | 8.9 | 8.2 ± 0.4 | 20.2 | 15.16 ± 0.75 | 9.34 ± 0.43 |
14 | WR | He ii | 4541 | 24.6 | 4541.0 | 5.19 ± 0.45 | 29.9 | 7.8 ± 0.7 | 20.2 | 14.36 ± 1.25 | 8.89 ± 0.73 |
15 | WR | C iv | 4789 | 64.5 | 4789.2 | 1.99 ± 0.33 | 21.4 | 3.4 ± 0.6 | 20.2 | 5.51 ± 0.91 | 3.84 ± 0.62 |
16 | WR | O v | 4933 | 113.9 | 4933.1 | 4.87 ± 0.38 | 30.3 | 8.7 ± 0.7 | 20.2 | 13.48 ± 1.05 | 9.92 ± 0.74 |
17 | WR | O v | 5100 | 113.9 | 5100.0 | 3.60 ± 0.41 | 41.5 | 6.9 ± 0.8 | 20.2 | 9.96 ± 1.14 | 7.84 ± 0.86 |
18 | WR | O vi | 5166 | 138.1 | 5166.5 | 0.52 ± 0.06 | 11.4 | 1.0 ± 0.1 | 20.2 | 1.44 ± 0.17 | 1.15 ± 0.13 |
19 | WR | O vi | 5290 | 138.1 | 5288.9 | 13.13 ± 0.09 | 17.3 | 26.4 ± 0.2 | 66.8 | 36.33 ± 0.28 | 29.94 ± 0.09 |
20 | WR | He ii | 5412 | 24.6 | 5411.8 | 8.49 ± 0.09 | 23.6 | 17.9 ± 0.2 | 66.8 | 23.49 ± 0.26 | 20.34 ± 0.13 |
21 | WR | C iv | 5470 | 64.5 | 5468.6 | 6.89 ± 0.10 | 26.6 | 114.9 ± 0.2 | 66.8 | 19.07 ± 0.26 | 16.91 ± 0.15 |
22 | WR | O v | 5600 | 113.9 | 5595.0 | 2.59 ± 0.07 | 35.5 | 5.9 ± 0.2 | 65.5 | 7.17 ± 0.28 | 6.72 ± 0.22 |
23 | WR | O vi | 6200 | 138.1 | 6198.5 | 3.35 ± 0.08 | 19.0 | 10.2 ± 0.3 | 43.3 | 9.27 ± 0.22 | 11.61 ± 0.24 |
24 | WR | He ii | 6406 | 24.6 | 6406.0 | 0.63 ± 0.03 | 11.8 | 2.2 ± 0.2 | 43.3 | 1.74 ± 0.14 | 2.51 ± 0.20 |
25 | WR | He ii | 6560 | 24.6 | 6557.7 | 10.95 ± 0.07 | 44.5 | 36.7 ± 0.4 | 43.3 | 30.30 ± 0.35 | 41.69 ± 0.29 |
26 | WR | O v | 6740 | 113.9 | 6746.3 | 1.33 ± 0.10 | 47.9 | 5.3 ± 0.4 | 43.3 | 3.68 ± 0.26 | 6.01 ± 0.40 |
27 | WR | C iv | 7060 | 64.5 | 7059.9 | 8.54 ± 0.04 | 35.4 | 39.0 ± 0.3 | 57.9 | 23.63 ± 0.18 | 44.31 ± 0.15 |
Special lines|$^{\dagger }\, ^{\dagger }$| | |||||||||||
28 | stellar emission | Ne vii | 4555 | 207.3 | 4552.5 | 1.14 ± 0.30 | 14.4 | 1.7 ± 0.5 | 20.2 | 3.15 ± 0.83 | 1.96 ± 0.51 |
29 | stellar emission | Ne vii | 5666 | 207.3 | 5665.4 | 1.63 ± 0.07 | 20.4 | 3.8 ± 0.2 | 65.5 | 4.51 ± 0.19 | 4.36 ± 0.17 |
30 | stellar emission | Ne viii | 6068 | 239.1 | 6065.9 | 1.51 ± 0.07 | 12.1 | 4.2 ± 0.2 | 43.3 | 4.18 ± 0.19 | 4.82 ± 0.21 |
(1) Identification number; (2) nature of the contributing emission line: WR (broad/stellar) or nebular (narrow); (3) ion; (4) rest wavelength in Å; (5) Ionization potential [eV]; (6) observed centre of the line; (7) flux [10−14 erg cm−2 s−1]; (8) full width at half-maximum (FWHM) [Å]; (9) equivalent width (EW) [Å]; (10) continuum signal-to-noise ratio (SNR) closest to the feature; (11) line fluxes normalized to that of the RB. The ratio has been computed adopting F(RB) = 100. (12) EW normalized to that of the RB, adopting EW(RB) = 100. Special lines |$^{\dagger }\, ^{\dagger }$| correspond to high ionization Ne lines from stellar emission origin (Werner, Rauch & Kruk 2007). † Only the statistical errors, determined with equations (1) and (2), are shown in this table.
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